Table 2.
Photometric and spectroscopic candidate redshifts.
| ID | zMUSE | zI17(a) | zBagpipes | BPZ (b) | zEAZY(b) |
|---|---|---|---|---|---|
| (3) | (4) | (5) | (6) | (7) | |
| F275W-314 | 1.995 | 1.995011 (3) | 2.09 ± 0.08 | 2.073 (0.99) | 1.825 (1.00) |
| F275W-2055 | – | – | 2.07 ± 0.08 | 2.430 (0.99) | 2.256 (1.00) |
| F336W-189 | 3.46 | 3.462787 (3) | 0.11 ± 0.05 | 3.313 (1.00) | 0.173 (1.00) |
| F336W-554 | – | 2.867758 (3) | 0.47 ± 0.05 | 2.972 (1.00) | 2.960 (1.00) |
| F336W-606 | – | – | 2.41 ± 0.15 | 2.69 (0.99) | 2.50 (1.00) |
| F336W-1013 | 2.98 | 2.981311 (2) | 2.04 ± 0.07 | 1.893 (0.99) | 1.811 (1.00) |
| F336W-1041 | – | 3.330044 (2) | 2.19 ± 0.09 | – | – |
| F336W-1041 | 3.329 | 3.329164 (2) | 2.19 ± 0.09 | 2.186 (0.99) | 2.004 (1.00) |
Notes. Redshifts calculated by various methods for objects of interest in our sample. Bold as in Table 1. BAGPIPES -computed redshifts are based on segment fluxes; updated BAGPIPES redshifts for F275W-2055 and F336W-606 based on larger apertures are reported below.
Numbers i parentheses are the confidence levels from I17 on a scale from 1–3, with higher being better.
Numbers in parentheses are the integrated probabilities (ODDS) reported by R15, where they are also explained (p. 9). According to Rafelski et al. (2015), a value of ≥0.9 is considered a high-probability determination.
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